TY - JOUR
T1 - New code for equilibriums and quasiequilibrium initial data of compact objects. IV. Rotating relativistic stars with mixed poloidal and toroidal magnetic fields
AU - Uryu, Koji
AU - Yoshida, Shijun
AU - Gourgoulhon, Eric
AU - Markakis, Charalampos
AU - Fujisawa, Kotaro
AU - Tsokaros, Antonios
AU - Taniguchi, Keisuke
AU - Eriguchi, Yoshiharu
N1 - Funding Information:
This work was supported by JSPS Grant-in-Aid for Scientific Research(C) Grants No. 18K03624, No. 15K05085, No. 18K03606, and No. 17K05447; NSF Grant No. PHY-1662211; NASA Grant No. 80NSSC17K0070; and the Marie Sklodowska-Curie Grant No. 753115. APPENDIX A:
Publisher Copyright:
© 2019 American Physical Society.
PY - 2019/12/19
Y1 - 2019/12/19
N2 - A new code for computing fully general relativistic solutions of strongly magnetized rapidly rotating compact stars is developed as a part of the Compact Object CALculator (cocal) code. The full set of Einstein's equations, Maxwell's equations, and magnetohydrodynamic equations are consistently solved assuming perfect conductivity, stationarity, and axisymmetry, and strongly magnetized solutions associated with mixed poloidal and toroidal components of magnetic fields are successfully obtained in generic (noncircular) spacetimes. We introduce the formulation of the problem and the numerical method in detail, then present examples of extremely magnetized compact star solutions and their convergence tests. It is found that, in extremely magnetized stars, the stellar matter can be expelled from the region of strongest toroidal fields. Hence, we conjecture that a toroidal electrovacuum region may appear inside of the extremely magnetized compact stars, which may seem like the neutron star becoming the strongest toroidal solenoid coil in the Universe.
AB - A new code for computing fully general relativistic solutions of strongly magnetized rapidly rotating compact stars is developed as a part of the Compact Object CALculator (cocal) code. The full set of Einstein's equations, Maxwell's equations, and magnetohydrodynamic equations are consistently solved assuming perfect conductivity, stationarity, and axisymmetry, and strongly magnetized solutions associated with mixed poloidal and toroidal components of magnetic fields are successfully obtained in generic (noncircular) spacetimes. We introduce the formulation of the problem and the numerical method in detail, then present examples of extremely magnetized compact star solutions and their convergence tests. It is found that, in extremely magnetized stars, the stellar matter can be expelled from the region of strongest toroidal fields. Hence, we conjecture that a toroidal electrovacuum region may appear inside of the extremely magnetized compact stars, which may seem like the neutron star becoming the strongest toroidal solenoid coil in the Universe.
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U2 - 10.1103/PhysRevD.100.123019
DO - 10.1103/PhysRevD.100.123019
M3 - Article
AN - SCOPUS:85077356680
SN - 2470-0010
VL - 100
JO - Physical Review D
JF - Physical Review D
IS - 12
M1 - 123019
ER -